no slide title - nasa...5 modes of data collection • survey: modes 1 & 3 • ssa: supported...

National Aeronautics and Space Administration

MCATMeter Class Autonomous Telescope

Dr. Sue Lederer

Orbital Debris Program Office

https://ntrs.nasa.gov/search.jsp?R=20160003853 2020-04-19T16:40:16+00:00Z


NASA/AFRL joint project

• NASA– Principal Investigator: Dr. Susan Lederer– Project Management & Logistics: Lisa Pace– ODPO Office: Gene Stansbery– JETS contractor staff: Dr. Heather Cowardin, Dr. Brent Buckalew, Dr. James Frith

• Air Force Research Laboratory (AFRL)– Schafer Corp: Hardware integration: Tom Glesne– Pacific Defense Solutions, Integrity Applications Inc.: Riki Maeda, Dennis Douglas,

Daron Nishimoto– AFRL Maui: Paul Kervin– Air Force Nuclear Weapons Center (AFNWC):

• Architectural contract• Euclid Research/ U British Columbia

– Dr. Paul Hickson• Air Force 45th Space Wing

– Detachment 2 Ascension Auxiliary Airfield, Ascension Island– Cape Canaveral Air Force Station

• Construction contract


Optical and IR Telescopesused by the NASA debris office

UKIRT 3.8mMauna Kea

MCAT 1.3mAscension Island

MODEST 0.6mMagellan 6.5m (x2)

CTIO 4.0m


Location of NASA MCAT

(7o 58’ S; 14o 24’ W)~350’ Elevation; Google Earth Image)


Ascension Island


MCAT site

PrevailingWinds


Project Overview• Collaboration between NASA, Air Force 45th Space Wing, and Air Force Research

Laboratory (AFRL) Maui Optical Site (AMOS)

• MCAT Goal: Statistically characterize under-sampled orbital regimes– Geosynchronous and near GEO altitudes– LILO, i.e. Low inclination Low Earth Orbit (LEO)

• Evening and morning twilight – Share Metric Observations with DoD

• MCAT Objectives:– Monitor and assess orbital debris environment by surveying, detecting, and tracking orbiting

objects at:• LEO, MEO, GTO, GEO altitudes

• Debris as small as 20-30 cm in GEO should be detectable• GEO debris surveys

Share Obs with Air Force Space Command (AFSpC)

– May participate in JSpOC (Joint Space Operations Center) follow-up or hand-off activities

• Ascension Island location enables access to under-sampled low inclination orbits and new GEO longitudes

• Existing technical staff for “caretaker” support • Automated data analysis at site• Low data transmission requirements – transmit results, not data

(7o 58ʹ S, 14o 24ʹ W)


Operational Concepts to attain Objectives(BIG PICTURE)

• 5 Modes of data collection• Survey: Modes 1 & 3• SSA: supported most through modes 2 & 3

– Mode 2 to determine individual object characteristics/orbits– Mode 3 for rapid follow-up after break-up event

• Data to be transferred off island via DSCS

2. Catalog or Object-of-Interest

Tracking:

Target specific objects for testing or

characterization

1. GEO Sweep/ GEO Follow-up:

TDI mode matches GEO motion to sweep

GEO longitudes; follow-up specific targets for further characterization

3. Orbit Scan (LEO mode):

Define rate track by a given expected orbital

rate

5. Coordinated Observations:

I. Optical-OpticalminiCAT

II. Radar-OpticalC-band radar on

Ascension;

4. Stare –Detect –Chase:

Object crosses Field of View, its motion

calculated, chase at calculated rate of

motion


Meter Class Autonomous Telescope (MCAT)

• 1.3-m DFM telescope – 1.3m double horse-shoe DFM telescope

• Fast tracking smoothly through zenith– 7-m fast-tracking Observadome (GEODSS equivalent)– Spectral Instruments camera

• TDI (time-delay integration) enabled• 41ʹ x 41ʹ FOV (0.957° diagonal)• BVRI, gʹrʹiʹzʹ broadband filters

• 0.4m Mini-CAT• 16ʺ (0.4m) Officina Stellare telescope

Atlas focuser• LEO tracking Astelco mount• Finger Lakes Proline camera, e2V chip

• 44ʹ x 44ʹ FOV• 1.3ʺ per pixel (vs. 0.6ʺ/pix MCAT)

– Centerline Filterwheel• BVRI, gʹrʹiʹzʹ broadband filters

Simultaneous observations with MCAT in 2 filters (7° 58ʹ S, 14° 24ʹ W)


• Weather equipment– 5 weather station/sensors

• Temperature, Pressure• Wind speed average & direction• Humidity, dewpoint• Rain sensors• Cloud sensors

– All-Sky cam • View of the whole sky to determine cloud location and best observing strategy

– FLIR Infrared Cam (on MCAT)• 40deg FOV mounted on MCAT for real-time views of clouds as MCAT takes images

• Sky Brightness– Sky Brightness average (no moon): 21.3 – 21.7 mag/sq-arcsec

• Winds– 17-20mph average sustained winds, SE/SSE

• Seeing– Initial estimates: 1.5 – 2ʺ

Instrumentation:Weather, Clouds & All-Sky

National Aeronautics and Space AdministrationMCAT TimelineNew since IADC 2015: in bold

Systems Testing Construction Acceptance Testing

Full Integration/Data Collection

• July 2013: Telescope testing

• Aug 2013-June 2014: Software/Hardware integration testing

• Sept 2014, Ground-breaking

• Sept-March/April 2015: Main facility construction

• March-April 2015: Dome installation

• April-June 2015: Telescope installation

• Dec 2015: Begin fully integrated systems testing

• Jan 2016: Remote Data collection begin

• Apr/May 2015: miniCAT installation testing (16ʺ telescope)

• Full operations expected 20+ years

• June 2, 2015: Engineering First light

• June17: Camera failure• SAT for all except

Camera-specific tasks• Aug: 1st Light alt

camera for debris tracking, lightcurves

• Nov: Si Camera fix• Dec 2015: SI Camera


Instrument Commissioning

• Finger Lakes Fast-read out (alternate camera)– Originally purchased for the DIMM seeing monitor measurements– Electronically cooled (55C below ambient)– 3ʹ x 3ʹ FOV

• Small format, but fast read-out, electronic shutter (4 MHz or 10 MHz)• Lightcurve studies of known objects

– Instrument commissioning Aug 2015• SI camera (prime camera)

– Cryo-cooled (-110C)– Instrument commissioning Dec 2015– 41ʹ x 41ʹ FOV

• Survey, Object characterization

• FLIR Infrared sky-cam mounted on MCAT above secondary mirror


First Light: Aug 25, 2015FLI fast-readout camera

NGC 6302: The Bug Nebula GOES 4 Satellite Tracking


LEO pass of Transit 4a R/B debrisFLI fast-readout camera

• MCAT tracking LEO

• Animation (right)– FLI fast camera– 2015 Sept 03– ~10 second pass– 1 sec exposures– 2 images show star trails


Transit 4A Rocket Body

• First known satellite fragmentation– Ablestar stage successfully

deployed 3 payloads • Transit 4A• Injun• Solrad3

– LEO breakup, June 29,1961– 77 min after orbital insertion– Didn’t vent the remaining 100kg of

propellant upon payload separation– Fuel venting recommended after

this event!• Fragments cataloged

– 296 fragments cataloged– 181 still in orbit in 2008

Prime SI Camera Commissioning

Dec 2015


BRIZ-M Rocket Body Breakup Identified Jan 20, 2016

• Launched Dec 13, 2015, broke up 3:50 UTC Jan 16, 2016• Inserted into GEO orbit (33,400 x35,800km orbit)• Surveys to detect debris associated with the breakup cloud with

both MCAT and UKIRT

10-sec exposure in rʹ

Before

After


UKIRTUnited Kingdom Infrared Telescope

Mauna Kea, Hawaii


http://www.google.com/url?sa=i&rct=j&q=&esrc=s&source=images&cd=&cad=rja&uact=8&ved=0CAcQjRxqFQoTCITPi8yOosgCFcY5Pgod5vMIzA&url=http://apacificview.blogspot.com/2012/10/telescope-for-sale-one-careful-owner.html&psig=AFQjCNFI8UpJhrIwkJ___xDCcVkpMqLVZg&ust=1443817773840568

http://www.google.com/url?sa=i&rct=j&q=&esrc=s&source=images&cd=&cad=rja&uact=8&ved=0CAcQjRxqFQoTCITPi8yOosgCFcY5Pgod5vMIzA&url=http://apacificview.blogspot.com/2012/10/telescope-for-sale-one-careful-owner.html&psig=AFQjCNFI8UpJhrIwkJ___xDCcVkpMqLVZg&ust=1443817773840568


United Kingdom Infrared Telescope (UKIRT)

Thirty years of operations supporting advanced astronomical science.• UKIRT

• 3.8 meter telescope• One wide-field camera (0.8 sq. deg Field of view), 4 imager/spectrometer cameras• Optimized for near-mid infrared (0.8 – 25 μm)

• Location– Mauna Kea, Big Island, Hawaii: 13,800 feet (4200m) above sea level– Arguably the best ground based infrared observing location in the world


UKIRT Contract• UKIRT Management

– Lockheed Martin contract, PM Matt [email protected]

– PI: Rick Kendrick– U Arizona subcontract for daily operations

• NASA HQ Contract currently– Contract under HEOMD, Jason Crusan, COR– Principal Investigator and Technical COR:

Dr. Sue Lederer (NASA JSC)[email protected]

• Lockheed/Univ of Arizona is building a consortium of partners to support UKIRT

– Astronomical studies– Debris studies

mailto:[email protected]

mailto:[email protected]


UKIRT Instrumentation• Increases spectral and geographical coverage of GEO belt

• Instrumentation– Wide Field Camera: WFCam photometry

• ZYJHK (0.8-2.4 µm)– Two key Imager/spectrometers

• UIST (1-5 µm) • Michelle: (8-25 µm)

• IR + Vis photometry + albedo

– provides insight into material types and sizes

• Spectra– characterize surface material of orbital debris and targets of interest– Thermal characteristics

MCAT (vis) UKIRT - WFCAM


UKIRT Science• What can UKIRT do for us?

– UIST Spectrometer/Imager 0.85 – 5 μm• Near infrared absorption bands can be used to identify debris materials of

spacecraft by modeling with spectral database input Distinguish silicon band-gap signatures of Solar Panel near 1 μm

– Michelle spectrometer/imager 8 – 13 μm thermal imaging and spectra• Can be used to estimate size of debris

– WFCam (imager) & UIST spectrometer/imager 0.85 – 2.5 μm spectra• Space weathering study of HS-376 buses, cylinders covered in solar panels,

taken of satellites launched over a 2 decade window• GEO survey for debris population statistics• Survey of BRIZ-M rocket body Jan 16, 2016 breakup for 15 nights


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0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4

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Wavelength (µm)

SSN 12855 (SBS 2)

HS 376 bus

• Spectra can be used to determine materials comprising the observed object

• These buses are a good baseline to identify lines from solar panels

(Band gap from SilicateAbsorption fromSolar cells)

Known C-H bond features

water

C-H bond features


Rocket Body

C-H absorption

TelluricAbsorptionFrom AtmosphericWater vapor

• IUS Upper Stage– Carbon-carbon

epoxy– White paint– MLI

• 1.65 & 2.3 µm– C-H absorption– Indicative of

white paint

C-H absorption

https://www.google.com/imgres?imgurl=http://www.americaspace.com/wp-content/uploads/2014/10/sts34galileodeploy.jpg&imgrefurl=http://www.americaspace.com/?p%3D68949&docid=Nu1Kd-jd4oR3wM&tbnid=rJu4rrkIsJQcqM:&w=837&h=1038&ei=Kq3_VbehKc_UoAT8mRE&ved=0CAIQxiBqFQoTCLfewYDJh8gCFU8qiAod_EwEAA&iact=c&ictx=1

https://www.google.com/imgres?imgurl=http://www.americaspace.com/wp-content/uploads/2014/10/sts34galileodeploy.jpg&imgrefurl=http://www.americaspace.com/?p%3D68949&docid=Nu1Kd-jd4oR3wM&tbnid=rJu4rrkIsJQcqM:&w=837&h=1038&ei=Kq3_VbehKc_UoAT8mRE&ved=0CAIQxiBqFQoTCLfewYDJh8gCFU8qiAod_EwEAA&iact=c&ictx=1


Results: Data, Models, Residual

SatCom 1NEWSAT 1

R/B

UKIRT

IRTF

Ekran 2 Debris

IRTFIRTF Data from Abercromby et al. AMOS2015

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0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4

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Wavelength (µm)

SSN 12855 (SBS 2)UKIRT


HS 376 Bus Study:

• Investigating known shape/composition objects with respect to launch date Space weathering

Frith et al., Amos Tech. Conf. Proc. 2015


MSG Baffle Cover & Cooler Cover

vs UT

vs SolarPhaseAngle

Lederer et al., Amos Tech. Conf. Proc. 2014


UKIRT data taken by Debris office

• Dataset in hand– GEO near-IR survey data with WFCam imager (20 nights)– GEO target specific studies with WFCam near-IR imager (LOTS)

• HS-376 Rocket bodies• Titan and Ekran debris• Array covers, rocket bodies

– GEO/MEO near-IR Spectral studies (1-2.5µm)• HS-376 buses (cylinders surrounded by solar panels)• Dead satellites (buses with wings)• Rocket bodies• Debris: Titan, Ekran, Baffle and array covers• Etalon at MEO

– GEO/GTO Thermal IR studies – photometry and/or spectroscopy at 8-16 µm• HS376, buses with wings• Titan debris, Ariane debris

National Aeronautics and Space AdministrationAny Questions?


Backup slides


ODPO/MCAT Objectives (BIG PICTURE)

Primary:Distribution Function (#, size, type) for GEO-GTO* debris field

Achieved via sweep of inertial volume near GEO altitudes spanning inclinations expanded by solar lunar perturbations (stable plane).

Secondary: Debris type determination through multi-band (g′r′i′z′ or BVRI) photometric or spectroscopic

Rapidly respond to break-up event – time evolution of cloud

Distribution Function (#, size, type) for LEO-MEO* debris field extending to 0o inclination –achieved via static or orbit scan survey with subsequent trackingFast tracking telescope/dome can easily track Low Inclination Leo Objects (LILO)

*GEO = Geosync; HEO = High Earth Orbit; GTO = Geo Transfer Orbit; LEO = Low Earth Orbit; MEO = Middle Earth Orbit

Tertiary:SSA Coverage of Unique Longitude as contributing sensor of global sensor network –

Supports Space Situational Awareness (SSA) activities

Receive target Hand-offs from other global sensors – better orbit determination

Simultaneous Radar and Optical observations – in depth assessment of debris properties


• Distribution Function for GEO (GEO Survey)Achieved via sweep of inertial volume near GEO altitudes spanning inclinations expanded by solar lunar perturbations (stable plane). Patterned sweep is typically performed by counter-sidereal drift scan.

– DATA: (flux (#/brightness), size, classification)– MODE 1: Geo Survey / Geo Follow-up

• GEO Survey TDI mode: Telescope tracks at the Sidereal (star motion) rate and CCD scans

in the opposite direction (counter-sidereal) to track ‘motionless’ GEO objects Search via choosing selected phase angles and about the stable plane MCAT can track faster/slower during TDI mode for slightly different GEO orbits flux (number, brightness)

• GEO Follow-up Re-acquire GEO debris exhibiting longitudinal drift based on position/motion

from Survey mode Filter photometry material types

– Extension of MODEST program in Chile

MCAT Objectives: Primary


MCAT Objectives: Secondary• Rapid response to Break-up Event

Time evolution of cloud– DATA: (metrics, multiband filter photometry)– MODE 3: Orbit Scan

• Scan at the expected rate of the debris cloud• Define rate track by a given expected orbital rate of parent body• Discover daughter debris

Metrics orbital information Multiband filter photometry material type

• Debris type determination: Multi-band photometry (colors) or spectroscopy – DATA:(metrics, multiband filter photometry, [spectroscopy – future?])

• Eccentricity and orbital variations Area/Mass estimates Material type• Photometry/Spectroscopy Material type• Photometric lightcurves tumble rates, albedo variations

– MODE 2: Catalogue or Object of Interest Tracking in any orbit• Follows object of a known orbit to characterize colors or gather spectra for material type


MCAT adds this

unsampledregion

MCAT Performance at GEO• Limiting magnitude seen by other

telescopes around the world is dependent upon a variety of variables

– Atmospheric stability (seeing)– Site conditions (extinction due

to e.g. altitude, atmospheric aerosols)

– Telescope through-put– Filter chosen– Telescope mirror quality

• Assume MCAT experiences:– 1.5″ seeing on Ascension– Telescope encircled EE 70%– 18.9mag– 13cm at GEO assuming

0.175 albedo and very good atmospheric conditions

• miniCAT/RCAT/MAX– 16.5mag– 40 cm at GEO with 0.175

albedoMini/ MCATMax


CCD: Quantum EfficiencyFilters: BVRI and gʹrʹiʹzʹ

MCAT

miniCAT

no slide title - nasa...5 modes of data collection • survey: modes 1 & 3 • ssa: supported...

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